Mathematics
Scientific paper
Jan 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990phdt.......181w&link_type=abstract
Ph.D. thesis, Australian Natl. Univ., (1990)
Mathematics
6
Scientific paper
The Magellanic System is probed with a focus on the interactions in the System giving insight into the structure, dynamics and evolution of the Magellanic System. The past orbits of the Magellanic Clouds are modelled. A tidal encounter between the LMC and SMC has almost certainly occurred within the last 109 years. The observed structure of the Magellanic System supports this hypothesis and so it is accepted. This encounter event is found to be crucial to the understanding of the Magellanic System. Ca II absorption spectra of 25 Magellanic Cloud supergiants have been obtained at a resolution of 5 km s-1 using the Anglo-Australian Telescope. They are used with new H I observations from the Parkes radio telescope to reveal the three-dimensional structure of the Large and Small Magellanic Clouds. Radio continuum polarization maps of the LMC and SMC have been obtained at 2.3, 4.75 and 8.55 GHz using the Parkes telescope. They complement the optical polarization measurements in revelation of the magnetic field structure of the Magellanic Clouds. The gas in both Magellanic Clouds is seen to have a distance-velocity association. This breaks down south of 30 Doradus where the gas structure is complex. The radio and optical polarization measurements are seen to agree, indicating no significant line-of-sight structure to the aligned magnetic field in either the LMC or SMC. The pan-Magellanic field originally proposed by Mathewson and Ford finds support, and a clearly revealed spiral field centred on 30 Doradus merges smoothly with it. The Parkes telescope has been used to obtain finely gridded H I measurements of the Magellanic Stream and the high velocity H I around the Magellanic System. The origin of the intermediate velocity gas components seen in the direction of the LMC is finally determined. The Magellanic Stream is found to be bifurcated along its entire length with many anomalous velocity H I clouds alongside. A two component profile is discovered in the tip of the Stream indicating that nearby the extreme velocity clouds are part of the Stream. The high velocity clouds (HVCs) ahead of the Magellanic Stream are found to be part of a halo HVC population. The diffuse ram pressure origin of the Magellanic Stream is modelled. The origin of the Magellanic Stream is found to be the collision of a multi-phase halo (made up of the halo HVCs and diffuse corona) with the Inter-Cloud region. The popular tidal model for the origin of the Magellanic Stream fails to satisfy some of the important observational features and is thus rejected.
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